Data-driven model of the solar corona above an active region

Abstract

We aim to reproduce the structure of the corona above a solar active region as seen in the extreme ultraviolet (EUV) using a three-dimensional magnetohydrodynamic (3D MHD) model. The 3D MHD data-driven model solves the induction equation and the mass, momentum, and energy balance. To drive the system, we feed the observed evolution of the magnetic field in the photosphere of the active region AR 12139 into the bottom boundary. This creates a hot corona above the cool photosphere in a self-consistent way. We synthesize the coronal EUV emission from the densities and temperatures in the model and compare this to the actual coronal observations. We are able to reproduce the overall appearance and key features of the corona in this active region on a qualitative level. The model shows long loops, fan loops, compact loops, and diffuse emission forming at the same locations and at similar times as in the observation. Furthermore, the low-intensity contrast of the model loops in EUV matches the observations. In our model the energy input into the corona is similar as in the scenarios of fieldline-braiding or flux-tube tectonics, that is, energy is transported to the corona through the driving of the vertical magnetic field by horizontal photospheric motions. The success of our model shows the central role that this process plays for the structure, dynamics, and heating of the corona.

arXiv comment5 pages, 3 Figures, published in A&A letters

References in corpus (21)

• The stellar atmosphere simulation code Bifrost
• An Ab Initio Approach to the Solar Coronal Heating Problem
• Extension of the MURaM radiative MHD code for coronal simulations
• A Method for Data-Driven Simulations of Evolving Solar Active Regions
• Forward modeling of stellar coronae: from a 3D MHD model to synthetic EUV spectra
• An Ab Initio approach to Solar Coronal Loops
• Structure of solar coronal loops: from miniature to large-scale
• Coronal heating through braiding of magnetic field lines
• Bombs and flares at the surface and lower atmosphere of the Sun
• On red shifs in the transition region and corona
• Intermittent heating in the solar corona employing a 3D MHD model
• Solar Coronal Loops Associated with Small-scale Mixed Polarity Surface Magnetic Fields
• Constant cross section of loops in the solar corona
• Observationally driven 3D MHD model of the solar corona above an active region
• A model for the formation of the active region corona driven by magnetic flux emergence
• Nanoflare statistics in an active region 3D MHD coronal model
• Clusters of small eruptive flares produced by magnetic reconnection in the sun
• Limitations of force-free magnetic field extrapolations: revisiting basic assumptions
• Energetics of magnetic transients in a solar active region plage
• Coronal loops above an Active Region - observation versus model
• Current systems of coronal loops in 3D MHD simulations

Cited by in corpus (11)

• The Solar Orbiter mission -- Science overview
• Solar coronal heating from small-scale magnetic braids
• Is the High-Resolution Coronal Imager Resolving Coronal Strands? Results from AR 12712
• A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona
• A solar coronal loop in a box: Energy generation and heating
• An improved MHD simulation of the 2006 December 13 coronal mass ejection of active region NOAA 10930
• Data-Driven Radiative Magnetohydrodynamics Simulations with the MURaM code
• Stellar X-rays and magnetic activity in 3D MHD coronal models
• Magnetic Imaging of the Outer Solar Atmosphere (MImOSA): Unlocking the driver of the dynamics in the upper solar atmosphere
• Data-driven Radiative Magnetohydrodynamics Simulations with the MURaM Code: Coronal Heating and Dynamics in an Emerging Active Region
• Parallel plasma loops and the energization of the solar corona